Atomic and molecular interstellar medium in high redshift star-forming galaxies

高红移恒星形成星系中的原子和分子星际介质

• 批准号: 323130447
• 负责人: Professor Dr. Reinhard Genzel
• 金额: --
• 依托单位: Max-Planck-Institut für extraterrestrische Physik (MPE)
• 依托单位国家: 德国
• 项目类别: DIP Programme
• 财政年份: 2017
• 资助国家: 德国
• 起止时间: 2016-12-31 至 2020-12-31
• 项目状态: 已结题
• 来源: https://gepris.dfg.de/gepris/projekt/323130447?language=en
• 关键词: Atomic; molecular; interstellar; medium; redshift

Galaxies are the fundamental structural building blocks of the observable Universe. They contain the stars (and planets) together with the multi-phased, hot and cold, atomic and molecular interstellar medium (ISM) from which the stars themselves formed. Recent developments in observing technology for near-infrared and millimeter-wave imaging-spectroscopy have enabled breakthrough studies of the cosmologically cooled ISM in young high-redshift star-forming galaxies (SFGs). This includes the critical epochs when most of the mass was assembled in galaxies, through the rise, peak, and decline in the global cosmic star-formation rate. The molecular ISM is expecially important for the study of galaxy evolution because this material is most directly associated with star-formation. We propose a joint interdisciplinary observational/theoretical DIP program in Astrophysics for study of high-redshift galaxy and ISM evolution. Our program will be based on our already started and upcoming surveys, PHIBBS2 and ALMA-SFG for mm-wave spectroscopy at the advanced ground-based IRAM/NOEMA and ALMA interferometric arrays, in combination with near-IR KMOS3D with the ESO-VLT, to be followed by next-generation JWST observations from space. DIP/DFG funding will be used primarily for support of fundamental theory, development of analytic modeling tools and simulations. Key questions include: When and how did the (blue) SFG "main-sequence" become established? What determines the maximal "quenching mass" for star-forming galaxies? Is this due to shutdown of accretion from the surrounding hot medium and conversion to molecular gas? Or does internally generated feedback in the form of stellar or AGN wind-driven molecular/ionized outflows halt the galaxy growth rates? What are the star-forming and gaseous properties of galaxies transitioning to the (red) quiescent mode. How is angular momentum transferred from the galaxy halos to the stellar and gaseous disks? Does heavy element abundance ("metallicity") influence the star-formation efficiencies? Our theory and modeling work in coordination with our observing programs will be based on a series of work-packages especially designed with the training of young scientists in mind - undergrads, MSc/diploma, PhD students, and postdocs - bringing together a team of experts from the German and Israeli sides. Our research program will build on the established and internationally recognized German-Israel Astrophysics collaboration, led by the Genzel & Sternberg MPE-TAU partnership, for a major broadening of our research moving forward.

星系是可观测宇宙的基本结构组成部分。它们包含恒星（和行星）以及多相、热和冷、原子和分子的星际介质（ISM），恒星本身就是从这些星际介质形成的。近红外和毫米波成像光谱学观测技术的最新发展，使得对年轻高红移恒星形成星系（SFG）中宇宙学冷却的ISM的研究取得了突破性进展。这包括大部分质量聚集在星系中的关键时期，通过全球宇宙恒星形成率的上升，峰值和下降。分子ISM对于研究星系演化特别重要，因为它与恒星形成最直接相关。我们提出了一个联合的跨学科的观测/理论DIP计划在天体物理学的研究高红移星系和ISM的演变。我们的计划将基于我们已经开始和即将进行的调查，PHIBBS 2和ALMA-SFG在先进的地基IRAM/NOEMA和阿尔马干涉阵列上进行毫米波光谱学，结合近红外KMOS 3D和ESO-VLT，随后进行下一代JWST空间观测。DIP/DFG资金将主要用于支持基础理论、分析建模工具和模拟的开发。关键问题包括：（蓝色）SFG“主序列”是何时以及如何建立的？是什么决定了恒星形成星系的最大“淬灭质量”？这是由于周围热介质的吸积停止并转化为分子气体吗？还是内部产生的反馈，以恒星或活动星系核风驱动的分子/电离外流的形式，阻止了星系的增长速度？过渡到（红色）静止模式的星系的恒星形成和气体性质是什么？角动量是如何从星系晕转移到恒星盘和气体盘的？重元素丰度（“金属丰度”）是否影响恒星形成效率？我们的理论和建模工作与我们的观测计划相协调，将基于一系列的工作包，这些工作包特别为年轻科学家的培训而设计-本科生，硕士/文凭，博士生和博士后-汇集了来自德国和以色列的专家团队。我们的研究计划将建立在由Genzel &斯滕贝格MPE-TAU伙伴关系领导的已建立和国际公认的德国-以色列天体物理学合作的基础上，以进一步扩大我们的研究。